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Issue
A&A
Volume 640, August 2020
Article Number A101
Number of page(s) 10
Section The Sun and the Heliosphere
DOI https://doi.org/10.1051/0004-6361/202038348
Published online 21 August 2020

© ESO 2020

1. Introduction

Solar filaments are large magnetic structures confining cool and dense plasma suspended in the hot and tenuous corona. They are seen in absorption in Hα and extreme ultraviolet (EUV) channels when observed on the solar disk, and appear in emission and are described as “prominences” when observed above the solar limb (Mackay et al. 2010; Parenti 2014). A stable filament could erupt due to the loss of the balance of forces acting on them under several possible mechanisms, such as magnetic flux emergence and cancellation (Chen & Shibata 2000; Zhang et al. 2001; Su et al. 2011; Dacie et al. 2018), tether cutting reconnection (Moore et al. 2001; Chifor et al. 2007; Chen et al. 2014), breakout reconnection (Sterling & Moore 2004; DeVore & Antiochos 2008; Li et al. 2018), and ideal magnetohydrodynamic instability (Williams et al. 2005; Török & Kliem 2005; Hou et al. 2018; Zou et al. 2020). Filament eruptions are widely believed to play a critical role in the onset of solar flares and coronal mass ejections (CMEs; Lin & Forbes 2000; Chen 2011; Schmieder et al. 2013).

In two-dimensional (2D) eruption scenarios developed from the classical CSHKP model (Carmichael 1964; Sturrock 1966; Hirayama 1974; Kopp & Pneuman 1976), filament eruptions, solar flares, and CMEs are different observational manifestations of a more general single eruption process. It is well established that an erupting filament, usually lying above the magnetic polarity inversion line (PIL), stretches its overlying magnetic fields upward and forms a current sheet below, where magnetic reconnection occurs. If escaping successfully, this erupting filament will produce a CME into the interplanetary space. The particles accelerated by energy released through the reconnection propagate downward along the newly formed magnetic field and hit the lower solar atmosphere, producing two bright flare ribbons on both sides of the PIL (Priest & Forbes 2002; Shibata & Magara 2011; Hou et al. 2016). With the progress of the reconnection, new groups of field lines successively form with their altitudes increasing and brightened footpoints (the flare ribbons) apparently separating from each other. Therefore, the morphology and evolution of flare ribbons or brightenings in the lower solar atmosphere can provide significant insights into the topology and reconfiguration of magnetic systems during the solar eruption process (Savcheva et al. 2015; Qiu et al. 2017; Li et al. 2017a). Moreover, coronal dimmings (or transient coronal holes), regions characterized by abrupt emission reduction in EUV and soft X-ray (SXR) channels, are another distinct phenomenon associated closely with these solar eruptions (Hudson et al. 1996; Sterling & Hudson 1997; Zarro et al. 1999; Harrison et al. 2003; Jiang et al. 2011; Zhang et al. 2017; Veronig et al. 2019). In a recent series of works, two different types of coronal dimmings are distinguished: core and secondary (Mandrini et al. 2007; Dissauer et al. 2018a,b). The core dimmings are localized regions with an impulsive density decrease of up to 50%–70% within half an hour and do not replenish for more than 10 hours, whereas the secondary dimmings are more shallow and widespread regions that evolve more gradually and starts to recover after 1–2 hours (Vanninathan et al. 2018). The core dimmings are interpreted as the footpoints of erupting magnetic flux ropes, while the secondary dimmings are believed to be caused by the stretch and partial reconnection of overlying fields (Attrill et al. 2007; Mandrini et al. 2007; Dissauer et al. 2018b).

In addition to the single eruption mentioned above, the Sun also ubiquitously breeds sympathetic eruptions, which are defined as causally linked eruptions occurring with a relatively short time interval in different, but physically related source regions (Wang et al. 2001; Moon et al. 2002; Wheatland & Craig 2006; Schrijver & Title 2011; Titov et al. 2012). Observational and numerical works suggest that the physical linkages between the sympathetic eruptions should essentially be of a magnetic nature (Ding et al. 2006; Török et al. 2011; Wang et al. 2016). For example, sympathetic eruptions of two filaments are believed to be caused by the reconnection-related changes of background magnetic fields. Due to impacts from a nearby erupting filament, constraint fields above the other stable filament would be sufficiently removed (Shen et al. 2012; Lynch & Edmondson 2013; Joshi et al. 2016; Wang et al. 2018). The reconnection between the overlying fields applied in this scenario is virtually the same as the concept of external magnetic reconnection in the break-out model (Antiochos et al. 1999; Sterling & Moore 2004; Karpen et al. 2012; Zhou et al. 2017, 2019). The external reconnection occurs above the erupting field (e.g., magnetic flux rope) and not below it as depicted by the classical 2D CSHKP model, and thus produces various distinctly different observational features. In a broader meaning, other than between two sets of overlying fields, the external reconnection can also refer to the magnetic reconnection occurring between one erupting magnetic flux rope and its overlying arcades (Li et al. 2018; Yang et al. 2019a; Lörinčík et al. 2019; Chen et al. 2019a). Such an external reconnection geometry is consistent with the configuration of three-dimensional (3D) “ar-rf” reconnection, which occurs between the leg of an eruptive flux rope and neighboring inclined arcades (Aulanier & Dudík 2019).

To verify the sympathetic eruption scenario requiring the occurrence of external reconnection, it is necessary to find evidence from three aspects as follows: pre-existing magnetic topology in favor of occurrence of the reconnection, observational features of the reconnection when it happens, and the resultant reconfiguration of background fields. Although previous works reported some supportive clues such as a null point between two filaments involved in sympathetic eruptions (Zuccarello et al. 2009; Li et al. 2017b), pre-eruption coronal dimming appearing on both sides of the filament (Jiang et al. 2011; Wang et al. 2018), and bright ribbons detected around the stable filament (Joshi et al. 2016; Wang et al. 2018), a detailed analysis with an integrated evidence chain for the sympathetic eruptions of two filaments has rarely been proposed. Aiming to find the causal link between sympathetic eruptions of two filaments, Song et al. (2020) reported a sympathetic event involving successive eruptions of two filaments (F1 and F2). They provided a qualitative description about the causal link between the sympathetic eruptions of F1 and F2: the southwest ribbon formed from eruptive F1 invaded F2 from its southeast region with weaker overlying magnetic fields relative to its northwest region, disturbing F2 and leading F2 to eventually erupt. However, due to the lack of observational evidence of the interaction between erupting F1 and pre-eruption F2 and of the magnetic topology change during the sympathetic eruptions, some questions still remained to be answered: How did the southwest ribbon formed by eruptive F1 “invade” pre-eruption F2? and How did this intruding flare ribbon disturb F2 and then lead F2 to the eventual eruption? To obtain more insight into the specific physical process of the interaction between erupting F1 and pre-eruption F2, and the decisive factor of the subsequent eruption of F2, further analysis of more observational evidence and evolution of magnetic topology needs to be performed in a second study.

In the present work we investigate the same event as reported by Song et al. (2020) and present integrated evidence for the sympathetic process from the aspects of magnetic topology before reconnection, signatures during reconnection, and results after reconnection. The data from the Solar Dynamics Observatory (SDO; Pesnell et al. 2012) and other observatories are analyzed to reveal kinematic evolutions of the filaments, various observational signatures formed by the reconnection and the reconfiguration of overlying fields during the sympathetic eruptions. Based on more thorough nonlinear force-free field (NLFFF) extrapolations with a time sequence, we reveal the magnetic topology above the two filaments and its evolution that lead to various features during the eruptions. A more complete and concrete physical scenario is depicted in the present work to restore the realistic process of the interaction between the two filaments and the subsequent eruption of F2.

The remainder of this paper is structured as follows. Section 2 describes the observations and methods of data analysis taken in our study. In Sect. 3 the results of observations and analysis are presented and discussed. Finally, we summarize the major findings in Sect. 4.

2. Observations and data analysis

The sympathetic eruptions of the two filaments (F1 and F2) occurred on 2015 November 15-16 and were well observed by the SDO. The Atmospheric Imaging Assembly (AIA; Lemen et al. 2012) on board the SDO provides successive observations of the multilayered solar atmosphere in ten channels, including seven EUV passbands with a cadence of 12 s and a spatial resolution of 1.″5. The SDO/Helioseismic and Magnetic Imager (HMI; Schou et al. 2012) offers one-arcsecond resolution full-disk intensitygrams, line-of-sight (LOS) magnetograms, and Dopplergrams every 45 s, and photospheric vector magnetograms at a cadence of 720 s. Here we mainly analyze the AIA 304 Å, 171 Å, 193 Å, 211 Å, 335 Å, 94 Å, 131 Å images, the HMI LOS magnetograms, and the photospheric vector magnetograms. Moreover, Hα observations from the Global Oscillation Network Group (GONG; Harvey et al. 1996), solar corona images taken by the Large Angle and Spectrometric Coronagraph (LASCO; Brueckner et al. 1995) on board the SOHO, and the SXR 1–8 Å flux from the GOES are also employed.

Based on the almost simultaneous observations of six AIA EUV channels (131 Å, 94 Å, 335 Å, 211 Å, 193 Å, and 171 Å), we perform the differential emission measure (DEM) analysis based on the code xrtdemiterative2.pro in the Solar Software package (Weber et al. 2004). After being modified slightly, this method has been proved to work well with AIA data for retrieving the plasma DEM (Cheng et al. 2012). The total emission measure (EM) in temperature range Tmin ≤ lgT ≤ Tmax then can be calculated as follows:

(1)

The density n in the structure of interest is evaluated as

(2)

where l is the LOS depth of the emission structure. As investigated in Su et al. (2018), it should be noted that the DEM solutions derived from the routine xrtdemiterative2.pro and from the other two popular codes, the regularized inversion code (Hannah & Kontar 2012) and the sparse inversion code (Cheung et al. 2015), cannot effectively constrain plasma DEM at flaring temperatures (i.e., showing a significant amount of plasma above 10 MK) with AIA data alone. In the present work we want to study, through the DEM analysis, the coronal dimming region, which is mostly formed by the evacuation of plasma with a quiet-Sun coronal temperature of several MK (Dissauer et al. 2018a). Considering that this temperature value is far below the threshold value of 10 MK, we believe the routine modified from xrtdemiterative2.pro could be safely applied to AIA data here for a rough estimate of DEM-derived parameters (e.g., density and temperature).

To understand the 3D magnetic fields above F1 and F2 before their eruptions, we utilize the “weighted optimization” method to perform NLFFF extrapolations (Wiegelmann 2004; Wiegelmann et al. 2012) based on the HMI photospheric vector magnetograms observed at 22:00 UT on November 15 and 00:00 UT on November 16. The NLFFF calculations are performed within a box of 600 × 552 × 512 uniformly spaced grid points (436 × 401 × 372 Mm3). Furthermore, we calculate the distribution of decay index, defined here as

(3)

where Bhp is the strength of the horizontal component of the potential field derived from potential-field source-surface model (PFSS; Schatten et al. 1969), and z denotes the radial height above the photosphere. Kliem & Török (2006) demonstrate that in an analytical model of torus instability, a toroidal current ring becomes unstable when the decay index of the external poloidal field (Bep) reaches a critical value of ∼1.5. However, due to the difficulty in isolating Bep, the horizontal component of the potential field (Bhp) is usually adopted as an approximation since Bhp is orthogonal to the axis of the toroidal current ring and thus can create downward J × B force (Démoulin & Aulanier 2010; Kliem et al. 2013; Wang et al. 2018).

3. Results and discussion

3.1. Overview of sympathetic eruptions of the two filaments

On 2015 November 15, F1 and F2 were located in the southwest quadrant of the solar disk, separated by a narrow region of negative polarity (see top panels of Fig. 1). Figure 1(c) shows that F1 lay above a polarity inversion line (PIL) region between active regions (ARs) 12452 and 12449, and F2 lay above a PIL within AR 12449. Around 21:30 UT, F1 began to rise, then accelerated, and eventually erupted southwestward in the plane of the sky (POS). The eruptive F1 produced a B7.8 two-ribbon flare (panels (a2) and (b2)) and a subsequent CME with a mean projected speed of 501 km s−1 and a width angle of 122° in the SOHO LASCO C2 coronagraph field of view (panel (d1)). At about 00:30 UT on November 16, F2 started to erupt partially and caused another B6.6 two-ribbon flare and a CME with a mean projected speed of 853 km s−1 and a width angle of 166° (bottom panels)1. The GOES SXR 1–8 Å flux variation in panel (a3) reveals that the two B-class flares caused by the successive eruptions of F1 and F2 peaked at 00:08 UT and 02:58 UT on November 16, respectively (also see the associated animation). The peak between them was caused by a flare occurring in AR 12454, far away from the region of interest.

thumbnail Fig. 1.

Overview of the sympathetic eruptions of two filaments on 2015 November 15-16. (a1)–(a3): Sequence of GONG Hα images displaying evolutions of the two filaments (F1 and F2). The red and blue contours in panels (a1)–(a2) outline the filament fragments of F1 and F2, respectively. Ribbons produced by eruptive F1 and F2 and remanent F2 are denoted by arrows in panels (a2)–(a3). The GOES SXR 1–8 Å flux variation overlaid in panel (a3) reveals two B-class flares caused by eruptions of the two filaments. (b1)–(b3): Corresponding composite images of SDO/AIA 131 Å, 304 Å, and 171 Å channels. (c): Corresponding SDO/HMI LOS magnetogram. (d1)–(d2): Difference images from SOHO/LASCO C2 showing two successive CMEs driven by the sympathetic eruptions of F1 and F2. An animation of Hα, AIA composite, and LASCO C2 images, covering 21:30 UT on November 15 to 03:54 UT on November 16, is available online.

Based on the closeness in both space and time of the two erupting filaments, we can interpret them as sympathetic eruptions. Studying the same event, Song et al. (2020) presented a detailed analysis of the F1 eruption process and concluded that it is caused by the flux cancellation within F1 channel (similar to the events reported by Zhang et al. 2001; Hong et al. 2011; Yang & Chen 2019; Yang et al. 2019b). They claimed that the non-uniformity of the magnetic fields above F2 could be responsible for the sympathetic eruption of F2. In the present work, focusing on more important observational evidence (e.g., inward-spreading brightening and dimming region on the south side of the pre-eruption F2, subsequent partial eruption of F2, and the bending structure formed between the erupting western part and the remaining eastern part of F2), we aim to reveal the specific physical process of the interaction between erupting F1 and pre-eruption F2 and the subsequent eruption of F2. The results in this work significantly supplement the former works about the sympathetic eruptions of filaments.

3.2. Inward-spreading brightening and coronal dimming on the south side of pre-eruption F2

The sequence of 304 Å images in Fig. 2(a1)–(a3) displays the evolution of eruptive F1 and the induced two flare ribbons. To intuitively exhibit the apparent motions of the two ribbons, we indicate the positions of newly brightened ribbons with different colors according to the time of their appearance and then superimpose them on one HMI LOS magnetogram (panel (a4)). The ribbons on both sides of the PIL related to F1 showed apparent separation motions, i.e., the northeast ribbon (NRF1) moved northeastward, and the southwest ribbon (SRF1) spread southwestward. It is remarkable that in the region outlined by the green square in panel (a3), when SRF1 approached F2, a relatively weak brightening (IBF2) was observed on the south side of F2 around 23:14 UT on November 15 and then kept spreading northward, inward approaching F2 (see panels (b1)–(b4) and associated animation). Panel (b4) indicates that from south to north, this inward-spreading brightening IBF2 swept regions with positive polarity on the south side of F2 and eventually stopped at a ribbon-shaped positive field close to F2. Behind IBF2, a distinct coronal dimming region was extending (panels (c1) and (c2)). Then around 23:54 UT, a bright cusp structure ahead of SRF1 and brightenings simultaneously appeared on opposite sides of F2 (green circles in panels (b3), (c1), and (c2)). Calculating the mean emission strength of 304 Å channel within regions N and S defined in panel (b1), we notice that the emission flux variations of the two regions closely match in the aspect of transient emission strengthening (colored regions in panel (d)). The synchronicity feature implies that the brightenings on opposite sides of pre-eruption F2 could result from the same physical process.

thumbnail Fig. 2.

Kinematic evolutions of eruptive F1 and the inward-spreading brightening on the south side of pre-eruption F2. (a1)–(a3): Sequence of AIA 304 Å images showing evolutions of F1 and two flare ribbons (NRF1 and SRF1). (a4): HMI LOS magnetogram superimposed with colored regions indicating positions of the evolving flare ribbons detected at different times in the 304 Å channel. (b1)–(b3): Enlarged 304 Å images displaying evolutions of SRF1 (dashed curves) and northward bright ribbon (IRF2) appearing on the south side of F2 (dotted curves). Green circles in (b3) indicate simultaneous brightenings on opposite sides of F2. (b4): Similar to (a4), but for the ribbons approaching F2 from two sides. (c1)–(c2): 171 Å and 131 Å images corresponding to (b3). (d): Variations in mean emission strength of the 304 Å passband within the regions N and S in (b1)–(b3). An associated animation of the 304 Å, 171 Å, and 131 Å images, covering 21:30 UT on November 15 to 00:30 UT on November 16, is available online.

As shown in Fig. 2(d), the emission flux of region S also presents an obvious decline after 23:10 UT, which could be attributed to the coronal dimming occurring on the south side of pre-eruption F2. Here we perform DEM analysis for the coronal dimming region based on observations of six AIA EUV channels and show the results of plasma density and temperature in Fig. 3. The dimming region outlined by the white curves in Fig. 1 was located above the region with positive polarity and underwent a noticeable density depletion after 23:10 UT on November 15 (panels (b1)–(b3)). Taking the mean value of plasma total EM in the dimming region as EM0 around 23:10 UT on November 15, we measure that the value then dramatically decreased to ∼0.5EM0 within 1 hour. Here we also employ the sparse inversion code (Cheung et al. 2015; Su et al. 2018) and find that this method gives similar results. According to Eq. (2), assuming the LOS depth l as a constant during the evolution of the dimming region, we can derive that the corresponding plasma density would decrease from n(t0) to . That is a density reduction of about 30% within 1 hour. We note that in the actual situation the LOS depth l could increase due to the stretch of magnetic fields and the expansion of the plasma in the dimming regions (Veronig et al. 2019). Thus, the value of 30% for the density reduction ought to be a lower limit. Additionally, panels (c1)–(c3) denote that the mean value of DEM-weighted average temperature in the dimming region changed from T0 to ∼0.9T0, only slightly decreasing by 10%. These results support the viewpoint that the coronal dimmings are primarily caused by mass expansion (or evacuation) and subsequent density depletion rather than temperature decrease (Hudson et al. 1996; Harra & Sterling 2001; Jin et al. 2009; Tian et al. 2012; Veronig et al. 2019).

thumbnail Fig. 3.

Coronal dimming on the south side of pre-eruption F2. (a1)–(a3): Sequence of AIA 193 Å images showing the appearance of coronal dimming on the south side of F2 before its eruption. The red and blue curves are contours of the HMI LOS magnetograms at ±50 G. The white curves outline the border of the dimming region around 00:10 UT on November 16. (b1)–(c3): Corresponding total EM and DEM-weighted average temperature maps exhibiting the evolution of plasma density and temperature in the dimming region. An associated animation of 193 Å images, covering 23:10 UT on November 15 to 00:10 UT on November 16, is available online.

Bright ribbons and coronal dimmings detected during solar eruptions essentially reflect the energy release and magnetic topology reconfiguration resulting from successive reconnection in the corona. The two ribbons showing apparent separation motions caused by the erupting F1 in this work can be explained by the reconnection beneath rising F1 in the standard flare model (Priest & Forbes 2002). However, the inward-spreading brightening IBF2 and subsequent dimming on the south side of pre-eruption F2, as well as the synchronicity of transient brightenings appearing on both sides of F2 ought to be attributed to a different physical mechanism: the external reconnection between the overlying fields above erupting F1 and stable F2 (Török et al. 2011). The concept of external reconnection was also applied in previous works to explain the EUV brightenings and coronal dimming near a pre-eruption filament (Jiang et al. 2011; Joshi et al. 2016; Li et al. 2017b; Wang et al. 2018). In the present work, the evolutions of inward-spreading brightening and its following coronal dimming beside the pre-eruption filament are unambiguously detected. They are very similar to the widespread secondary dimmings behind the diffuse bright fronts caused by the driven reconnections between the outer edge of an expanding CME magnetic field and quiet-Sun magnetic loops (Attrill et al. 2007; Mandrini et al. 2007). The brightenings on both sides of stable F2 could correspond to the footpoints of newly formed loops through the external reconnection between the magnetic fields above erupting F1 and stable F2. The dimming region behind the inward-spreading brightenings formed after the eruption of F1 but was located on the south side of pre-eruption F2. Compared with the core dimming region around the north footpoints of erupting F1 (not shown in the present work), this dimming region underwent a relatively slow density reduction of about 30%, which recovered soon after several hours. As a result, we speculate that this dimming region could be a secondary dimming and host footpoints of coronal arcades overlying F2, which reconnected with the expanding fields above erupting F1. This secondary dimming was produced by the reconnection-related magnetic fields reconfiguration, subsequent expansion or evacuation of plasma frozen in the coronal fields, and the resultant emission reduction. Additionally, it is also possible that this secondary dimming hosted footpoints of large-scale loops above F1 and F2, which were thus stretched by the erupting F1. For more detailed information about this process, an analysis of the magnetic topology above the two filaments is needed.

3.3. Quadrupolar magnetic topology with a null point above F1 and F2

To understand the magnetic topology that leads to the features shown in Figs. 2 and 3, we extrapolate 3D magnetic fields above F1 a nd F2 through NLFFF modeling based on the photospheric vector field of 22:00 UT on November 15, before the eruption of F1. Figure 4(a) reveals a quadrupolar system above F1 and F2, consisting of four magnetic connectivities (P1/N1 and P1/N2 above F1, P2/N2 and P2/N1 above F2). A large gradient in field line mapping is prominent in this system; for example, field lines emanating from P1 are at first parallel but then diverge significantly near their apexes, forming two sets of loops that are almost antiparallel with each other and connected to N1 (pink) and N2 (white), respectively. Field lines emanating from P2 have the same topology, forming two groups of structures (orange P2/N1 and green P2/N2). This magnetic topology strongly indicates the existence of a null point, which is further supported by the 3D distribution of magnetic field strength (panels (b)–(c)). Checking distribution of field strength in the vertical plane based on the dark blue curve marked in panel (a), we indeed find a possible null point situated at ∼90 Mm height (panel (d)). The corresponding decay index map (panel (e)) and the height profiles of decay index (panel (f)) reveal that in a limited altitude range near this null point, the decay index increases drastically, then impulsively decreases to a negative value, followed by a gradual positive recovery. These features are consistent with the existence of a null point, where the field strength becomes zero (Török & Kliem 2007).

thumbnail Fig. 4.

Three-dimensional (3D) magnetic fields above F1 and F2 revealed by NLFFF extrapolation at 22:00 UT on November 15. (a): Overlying loops of F1 and F2, forming a quadrupole magnetic field configuration. (b)–(c): Top view and side view of 3D distribution of magnetic field strength with values between 5 and 25 Gauss in the selected cube. (d)–(e): Distributions of magnetic field strength and decay index in the vertical plane based on the dark blue cut denoted in (a). The null point of the quadrupole magnetic configuration is distinctly depicted at a height of ∼90 Mm. (f): Height profiles of decay index averaged within two regions defined by two blue lines and two red lines in the vertical plane of (e), respectively.

Furthermore, we perform NLFFF extrapolation based on the photospheric vector field of 00:00 UT on November 16, when the ribbon SRF1 produced by erupting F1 approached stable F2, and inward-spreading brightening and coronal dimming appeared on the south side of pre-eruption F2. The extrapolation results shown in Fig. 5 reveal that at that time, the quadrupolar system still existed there, but the null point moved southwestward in the POS. Furthermore, the height of the null point had decreased from ∼90 Mm to ∼40 Mm.

thumbnail Fig. 5.

NLFFF extrapolation results derived from the photospheric vector field of 00:00 UT on November 16.

3.4. Physical scenario of the sympathetic eruption of F1 and F2: External reconnection and subsequent reconfiguration of the overlying magnetic fields

The quadrupolar configuration with a possible null point above F1 and F2 revealed by the field extrapolation is favorable for magnetic reconnection (Aschwanden et al. 1999; Sun et al. 2012). We infer that this configuration facilitates the sympathetic eruptions of F1 and F2 as follows. As reported by Song et al. (2020), the eruption of F1 was triggered by the flux cancellation within the F1 channel. Reconnection then occurred beneath the erupting F1 and produced two flare ribbons as shown in Figs. 1 and 2 (also see the associated animations). The rising F1 kept pushing its overlying magnetic fields upward (with a POS component to the southwest), approaching the overlying fields of stable F2 under the quadrupolar configuration shown in Fig. 4(a). Then the external magnetic reconnection occurred between pink P1/N1 above F1 and green P2/N2 above F2 near the null point, forming new loops connecting P2 and N1. Then brightenings on both sides of stable F2 appeared around the footpoints of these newly formed loops and showed good synchronicity (Fig. 2(d)). As the external reconnection went on, the fields above F2 would be involved gradually from the outside to the inside (lower and lower in height), manifesting as the inward-spreading brightening in lower atmosphere shown in Fig. 2 (corresponding to footpoint motion of the field lines formed by the external reconnection). In addition, the external reconnection would also reconfigure the overlying fields of F2 as follows: transporting magnetic flux from P2/N2 (green curves in Fig. 4(a)) to P2/N1 (orange curves), weakening confinement above the west part of F2, and reinforcing confining fields above the east part of F2. Since the magnetic flux in system P2/N2 was gradually reduced in a fixed sized space, in terms of magnetic flux density this process was equivalent to the expansion of magnetic system P2/N2, which usually produced the secondary coronal dimming (Mandrini et al. 2007; Dissauer et al. 2018b). As a result, the plasma frozen in magnetic loops P2/N2 around the positive footpoints, which were within the dimming region (see Figs. 3(a3) and 4(a)), would be gradually evacuated outward from this region. Then, the plasma density of the region above the positive footpoints of P2/N2 kept decreasing, and a secondary coronal dimming was gradually extending there, behind the inward-spreading brightening (Figs. 2 and 3).

Consistent with the physical scenario proposed above, in the quadrupolar system revealed by the NLFFF extrapolation at 00:00 UT on November 16, the null point moved southwestward in the POS and had a lower height than about 2 hours earlier (comparing Fig. 4 with Fig. 5). It indicates that the field above erupting F1 (pink curves in Figs. 4 and 5) kept approaching the overlying fields of F2 (green curves), leading to successive external reconnection around the null point. As the reconnection continued, the outermost layer of the fields above F1 and F2 would be removed gradually, and the height of the reconnection site as well as the null point kept decreasing.

Moreover, the reconfiguration of overlying fields of F2 is further supported by the observations that F2 eventually underwent a partial eruption (Fig. 6 and the associated animation). Suffering impacts from the erupting F1, the west part of F2 started to rise slowly from 00:30 UT on November 16. Around 02:00 UT, the west part of F2 went through a robust acceleration and successfully erupted southwestward in the POS (Fig. 6(a)), producing two flare ribbons (panels (b) and (c)). However, at the east part of F2, the filament material was activated but confined within the filament channel and then moved southeastward (panels (c)–(e)). It is notable that during the rapid rising phase of F2, a bending structure appeared in its middle part (panels (b), (d), and (e)). The difference image of the 304 Å channel clearly depicts the bending axis of F2 (white curve in panel (f)). Moreover, the velocity fields derived from LCT method show that filament material in the bending region has two apparent motion patterns: a northward one and a southward one. Here we suggest that as a result of the aforementioned reconnection-related reconfiguration of the overlying fields, the eruption of the east part of F2 was blocked by its enhanced overlying fields, thus forming a bending structure between itself and the successfully erupting west part where the overlying fields were significantly weakened. The material within the bending region fell to the east part of F2 and then flowed along the remanent filament fields. The time-distance plots in Fig. 6(g)–(h) show that the west part of F2 eventually erupted with a POS velocity of 140 ± 6 km s−1, while the material in the east part moved along the filament axis after being activated.

thumbnail Fig. 6.

Partial eruption of F2. (a)–(c): 304 Å and Hα images showing partial eruption of F2. Green arrows in (a) denote eruptive direction of the west part of F2. Green ellipse in (b) marks a bending structure in the middle part of F2 during its rapid rising phase. White curves in (a)–(b) delineate the axis of eruptive F2. (d)–(f): 131 Å, 171 Å images, and difference image of 304 Å corresponding to (b). Green arrows in (d) and (e) represent southeastward motion of the activated material of the east part of F2. The colored arrows in (f) represent the horizontal velocity fields of filament material with values larger than 30 km s−1 derived from 304 Å images through LCT method. (g)–(h): Time-distance plots derived from the 304 Å images along lines “A–B” and “C–D” shown in (a). The dotted oblique line in (g) delineates linear fitting of the front of eruptive F2 in its rapid rising phase. An associated animation of 304 Å, 171 Å, and 131 Å images, covering 23:50 UT on November 15 to 03:59 UT on November 16, is available online.

Owing to the temporal overlap with the eruption of F1, projection effect, and that the external reconnection is expected to be relatively weak, we note that the observational signatures during the external reconnection process, such as the quasi-periodic pulsation (QPP) around the reconnection moment (Zhou et al. 2019; Chen et al. 2019b) or emission enhancements in EUV and X-ray channels (Yan et al. 2018; Zou et al. 2020) near the possible null point, are difficult to distinguish unambiguously from dominant features caused by the robust reconnection beneath erupting F1 in this event. Moreover, the loops corresponding to the overlying fields P1/N1, P2/N2, and newly formed P2/N1 were also not distinct in the AIA imaging observations. The absence of these loops could be caused by the weakness of the overlying fields and the external reconnection occurring between them. Although we have detected and analyzed some pieces of important evidence, which could constitute an integrated chain to support the occurrence of the external reconnection, the scenario proposed in the present work ought to be regarded as one alternative rather than an exclusive explanation, due to the absence of the observational signatures mentioned above. For example, the secondary coronal dimming reported here could also host footpoints of large-scale loops above F1 and F2, which were stretched by the erupting F1 and caused the formation of the secondary dimming.

4. Summary

We summarize our results as follows:

  1. On 2015 November 15-16, two filaments (north F1 and south F2) separated by a narrow region of negative polarity successively erupted, showing distinct sympathetic characteristics. The eruption of each filament was associated with a B-class flare and a CME.

  2. When the southward-spreading ribbon (SRF1) produced by first-erupting F1 approached stable F2, a relatively weak brightening (IBF2) was observed on the south side of F2 and then kept spreading northward, inward approaching F2. Moreover, brightenings could be detected on both sides of F2 and showed good synchronicity.

  3. Behind the inward-spreading brightening, a distinct secondary coronal dimming region was extending, where the mean value of plasma density decreased by about 30% and that of temperature declined by 10%.

  4. NLFFF extrapolations reveal that the fields above pre-eruption F1 and F2 constituted a quadrupolar magnetic system with a possible null point. Moreover, the null point kept moving toward F2 and descending within the following hours.

  5. F2 eventually partially erupted and formed a bending structure between the erupting west part and the remaining east part, which indicated non-uniform distribution of the constraint fields above F2.

  6. We propose that the rising F1 pushed its overlying fields toward the fields above stable F2 and caused successive external reconnection near the null point, resulting in simultaneous brightenings on both sides of stable F2 and the motion of the null point. From outside to inside (lower and lower in height), the fields above pre-eruption F2 were gradually involved in the reconnection, manifesting as the inward-spreading brightening and dimming on the south side of F2. The external reconnection could then reconfigure the confining fields above F2, resulting in its subsequent partial eruption.

The event analyzed here presents abundant sympathetic characteristics. Focusing on important observational evidence (e.g., the inward-spreading brightening and secondary dimming region on the south side of the pre-eruption F2, the subsequent partial eruption of F2, and the bending structure formed between the erupting west part and the remained east part of F2), we aim to reveal specific physical process of the interaction between erupting F1 and pre-eruption F2 and the subsequent eruption of F2. Based on more thorough NLFFF extrapolations with a time sequence, a quadrupolar magnetic system with a possible null point above the two filaments and its evolution are revealed. Here we report the evolution of the inward-spreading brightening and secondary coronal dimming beside the pre-eruption filament, reconfiguration of the quadrupolar magnetic system with a possible null point, a shift of the null-point to a lower altitude, and the resultant partial eruption of F2 during the sympathetic eruptions of two filaments. From the aspects of pre-existing magnetic topology in favor of reconnection, observational evidence of the external reconnection, and the reconnection-related reconfiguration of overlying fields, we propose an integrated evidence chain to unambiguously demonstrate the key roles of external magnetic reconnection between overlying fields and the resultant reconfiguration of magnetic topology on the sympathetic eruptions of two filaments. The characteristics of emission and magnetic topology investigated in the present work should be taken into account when studying the sympathetic eruptions of two filaments in future works.

1

More information about the CMEs related to the reported event is available in the SOHO LASCO CME catalog (Yashiro et al. 2004), https://cdaw.gsfc.nasa.gov/CME_list/.

Acknowledgments

The authors are grateful to the anonymous referee for the constructive suggestions improving this paper. Y. H. appreciates Dr. Shuhong Yang, Dr. Xiaoshuai Zhu, and Dr. Shuo Yang for valuable discussions. The data are used courtesy of SDO, GONG, SOHO, and GOES science teams. SDO is a mission of NASA’s Living With a Star Program. This work is supported by the Strategic Priority Research Program of the Chinese Academy of Sciences (XDB41000000), the National Natural Science Foundation of China (11903050, 11790304, 11773039, 11533008, 11873059, 11673035, 11673034, and 11790300), the National Key R&D Program of China (2019YFA0405000), the NAOC Nebula Talents Program, the Youth Innovation Promotion Association of CAS, Young Elite Scientists Sponsorship Program by CAST (2018QNRC001), and Key Programs of the Chinese Academy of Sciences (QYZDJ-SSW-SLH050). Z. S. acknowledges support from the open topic of the Key Laboratory of Solar Activities of the Chinese Academy of Sciences (KLSA201902).

References

  1. Antiochos, S. K., DeVore, C. R., & Klimchuk, J. A. 1999, ApJ, 510, 485 [Google Scholar]
  2. Aschwanden, M. J., Kosugi, T., Hanaoka, Y., et al. 1999, ApJ, 526, 1026 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  3. Attrill, G. D. R., Harra, L. K., van Driel-Gesztelyi, L., et al. 2007, ApJ, 656, L101 [NASA ADS] [CrossRef] [Google Scholar]
  4. Aulanier, G., & Dudík, J. 2019, A&A, 621, A72 [CrossRef] [EDP Sciences] [Google Scholar]
  5. Brueckner, G. E., Howard, R. A., Koomen, M. J., et al. 1995, Sol. Phys., 162, 357 [NASA ADS] [CrossRef] [Google Scholar]
  6. Carmichael, H. 1964, NASA Spec. Pub., 50, 451 [NASA ADS] [Google Scholar]
  7. Chen, H., Zhang, J., Cheng, X., et al. 2014, ApJ, 797, L15 [CrossRef] [Google Scholar]
  8. Chen, H., Yang, J., Ji, K., et al. 2019a, ApJ, 887, 118 [Google Scholar]
  9. Chen, P. F. 2011, Liv. Rev. Sol. Phys., 8, 1 [Google Scholar]
  10. Chen, P. F., & Shibata, K. 2000, ApJ, 545, 524 [Google Scholar]
  11. Chen, X., Yan, Y., Tan, B., et al. 2019b, ApJ, 878, 78 [NASA ADS] [CrossRef] [Google Scholar]
  12. Cheng, X., Zhang, J., Saar, S. H., et al. 2012, ApJ, 761, 62 [NASA ADS] [CrossRef] [Google Scholar]
  13. Cheung, M. C. M., Boerner, P., Schrijver, C. J., et al. 2015, ApJ, 807, 143 [NASA ADS] [CrossRef] [Google Scholar]
  14. Chifor, C., Tripathi, D., Mason, H. E., et al. 2007, A&A, 472, 967 [Google Scholar]
  15. Dacie, S., Török, T., Démoulin, P., et al. 2018, ApJ, 862, 117 [Google Scholar]
  16. Démoulin, P., & Aulanier, G. 2010, ApJ, 718, 1388 [NASA ADS] [CrossRef] [Google Scholar]
  17. DeVore, C. R., & Antiochos, S. K. 2008, ApJ, 680, 740 [NASA ADS] [CrossRef] [Google Scholar]
  18. Ding, J. Y., Hu, Y. Q., & Wang, J. X. 2006, Sol. Phys., 235, 223 [Google Scholar]
  19. Dissauer, K., Veronig, A. M., Temmer, M., et al. 2018a, ApJ, 855, 137 [NASA ADS] [CrossRef] [Google Scholar]
  20. Dissauer, K., Veronig, A. M., Temmer, M., et al. 2018b, ApJ, 863, 169 [NASA ADS] [CrossRef] [Google Scholar]
  21. Hannah, I. G., & Kontar, E. P. 2012, A&A, 539, A146 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  22. Harra, L. K., & Sterling, A. C. 2001, ApJ, 561, L215 [Google Scholar]
  23. Harrison, R. A., Bryans, P., Simnett, G. M., et al. 2003, A&A, 400, 1071 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  24. Harvey, J. W., Hill, F., Hubbard, R. P., et al. 1996, Science, 272, 1284 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  25. Hirayama, T. 1974, Sol. Phys., 34, 323 [NASA ADS] [CrossRef] [Google Scholar]
  26. Hong, J., Jiang, Y., Zheng, R., et al. 2011, ApJ, 738, L20 [Google Scholar]
  27. Hou, Y., Zhang, J., Li, T., et al. 2016, ApJ, 829, L29 [NASA ADS] [CrossRef] [Google Scholar]
  28. Hou, Y. J., Zhang, J., Li, T., et al. 2018, A&A, 619, A100 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  29. Hudson, H. S., Acton, L. W., & Freeland, S. L. 1996, ApJ, 470, 629 [NASA ADS] [CrossRef] [Google Scholar]
  30. Jiang, Y., Yang, J., Hong, J., et al. 2011, ApJ, 738, 179 [Google Scholar]
  31. Jin, M., Ding, M. D., Chen, P. F., et al. 2009, ApJ, 702, 27 [NASA ADS] [CrossRef] [Google Scholar]
  32. Joshi, N. C., Schmieder, B., Magara, T., et al. 2016, ApJ, 820, 126 [Google Scholar]
  33. Karpen, J. T., Antiochos, S. K., & DeVore, C. R. 2012, ApJ, 760, 81 [NASA ADS] [CrossRef] [Google Scholar]
  34. Kliem, B., & Török, T. 2006, Phys. Rev. Lett., 96, 255002 [Google Scholar]
  35. Kliem, B., Su, Y. N., van Ballegooijen, A. A., et al. 2013, ApJ, 779, 129 [NASA ADS] [CrossRef] [Google Scholar]
  36. Kopp, R. A., & Pneuman, G. W. 1976, Sol. Phys., 50, 85 [NASA ADS] [CrossRef] [Google Scholar]
  37. Lemen, J. R., Title, A. M., Akin, D. J., et al. 2012, Sol. Phys., 275, 17 [Google Scholar]
  38. Li, S., Su, Y., Zhou, T., et al. 2017a, ApJ, 844, 70 [Google Scholar]
  39. Li, T., Zhang, J., & Hou, Y. 2017b, ApJ, 848, 32 [Google Scholar]
  40. Li, T., Yang, S., Zhang, Q., et al. 2018, ApJ, 859, 122 [NASA ADS] [CrossRef] [Google Scholar]
  41. Lin, J., & Forbes, T. G. 2000, J. Geophys. Res., 105, 2375 [NASA ADS] [CrossRef] [Google Scholar]
  42. Lörinčík, J., Dudík, J., & Aulanier, G. 2019, ApJ, 885, 83 [CrossRef] [Google Scholar]
  43. Lynch, B. J., & Edmondson, J. K. 2013, ApJ, 764, 87 [NASA ADS] [CrossRef] [Google Scholar]
  44. Mackay, D. H., Karpen, J. T., Ballester, J. L., et al. 2010, Space Sci. Rev., 151, 333 [NASA ADS] [CrossRef] [Google Scholar]
  45. Mandrini, C. H., Nakwacki, M. S., Attrill, G., et al. 2007, Sol. Phys., 244, 25 [NASA ADS] [CrossRef] [Google Scholar]
  46. Moon, Y.-J., Choe, G. S., Park, Y. D., et al. 2002, ApJ, 574, 434 [Google Scholar]
  47. Moore, R. L., Sterling, A. C., Hudson, H. S., et al. 2001, ApJ, 552, 833 [NASA ADS] [CrossRef] [Google Scholar]
  48. Parenti, S. 2014, Liv. Rev. Sol. Phys., 11, 1 [Google Scholar]
  49. Pesnell, W. D., Thompson, B. J., & Chamberlin, P. C. 2012, Sol. Phys., 275, 3 [Google Scholar]
  50. Priest, E. R., & Forbes, T. G. 2002, A&ARv, 10, 313 [NASA ADS] [CrossRef] [Google Scholar]
  51. Qiu, J., Longcope, D. W., Cassak, P. A., & Priest, E. R. 2017, ApJ, 838, 17 [NASA ADS] [CrossRef] [Google Scholar]
  52. Savcheva, A., Pariat, E., McKillop, S., et al. 2015, ApJ, 810, 96 [NASA ADS] [CrossRef] [Google Scholar]
  53. Schatten, K. H., Wilcox, J. M., & Ness, N. F. 1969, Sol. Phys., 6, 442 [Google Scholar]
  54. Schmieder, B., Démoulin, P., & Aulanier, G. 2013, Adv. Space Res., 51, 1967 [NASA ADS] [CrossRef] [Google Scholar]
  55. Schou, J., Scherrer, P. H., Bush, R. I., et al. 2012, Sol. Phys., 275, 229 [Google Scholar]
  56. Schrijver, C. J., & Title, A. M. 2011, J. Geophys. Res. (Space Phys.), 116, A04108 [Google Scholar]
  57. Shen, Y., Liu, Y., & Su, J. 2012, ApJ, 750, 12 [NASA ADS] [CrossRef] [Google Scholar]
  58. Shibata, K., & Magara, T. 2011, Liv. Rev. Sol. Phys., 8, 6 [Google Scholar]
  59. Song, Z., Hou, Y., Zhang, J., et al. 2020, ApJ, 892, 79 [Google Scholar]
  60. Sterling, A. C., & Hudson, H. S. 1997, ApJ, 491, L55 [Google Scholar]
  61. Sterling, A. C., & Moore, R. L. 2004, ApJ, 602, 1024 [Google Scholar]
  62. Sturrock, P. A. 1966, Nature, 211, 695 [NASA ADS] [CrossRef] [Google Scholar]
  63. Su, Y., Surges, V., van Ballegooijen, A., et al. 2011, ApJ, 734, 53 [Google Scholar]
  64. Su, Y., Veronig, A. M., Hannah, I. G., et al. 2018, ApJ, 856, L17 [CrossRef] [Google Scholar]
  65. Sun, X., Hoeksema, J. T., Liu, Y., et al. 2012, ApJ, 757, 149 [NASA ADS] [CrossRef] [Google Scholar]
  66. Tian, H., McIntosh, S. W., Xia, L., et al. 2012, ApJ, 748, 106 [Google Scholar]
  67. Titov, V. S., Mikic, Z., Török, T., et al. 2012, ApJ, 759, 70 [NASA ADS] [CrossRef] [Google Scholar]
  68. Török, T., & Kliem, B. 2005, ApJ, 630, L97 [Google Scholar]
  69. Török, T., & Kliem, B. 2007, Astron.e Nachr., 328, 743 [CrossRef] [Google Scholar]
  70. Török, T., Panasenco, O., Titov, V. S., et al. 2011, ApJ, 739, L63 [NASA ADS] [CrossRef] [Google Scholar]
  71. Vanninathan, K., Veronig, A. M., Dissauer, K., et al. 2018, ApJ, 857, 62 [Google Scholar]
  72. Veronig, A. M., Gömöry, P., Dissauer, K., et al. 2019, ApJ, 879, 85 [NASA ADS] [CrossRef] [Google Scholar]
  73. Wang, D., Liu, R., Wang, Y., et al. 2018, ApJ, 869, 177 [Google Scholar]
  74. Wang, H., Chae, J., Yurchyshyn, V., et al. 2001, ApJ, 559, 1171 [NASA ADS] [CrossRef] [Google Scholar]
  75. Wang, R., Liu, Y. D., Zimovets, I., et al. 2016, ApJ, 827, L12 [Google Scholar]
  76. Weber, M. A., Deluca, E. E., Golub, L., et al. 2004, Multi-wavelength Invest. Sol. Act. 321 [Google Scholar]
  77. Wheatland, M. S., & Craig, I. J. D. 2006, Sol. Phys., 238, 73 [Google Scholar]
  78. Wiegelmann, T. 2004, Sol. Phys., 219, 87 [NASA ADS] [CrossRef] [Google Scholar]
  79. Wiegelmann, T., Thalmann, J. K., Inhester, B., et al. 2012, Sol. Phys., 281, 37 [NASA ADS] [Google Scholar]
  80. Williams, D. R., Török, T., Démoulin, P., et al. 2005, ApJ, 628, L163 [NASA ADS] [CrossRef] [Google Scholar]
  81. Yan, X. L., Wang, J. C., Pan, G. M., et al. 2018, ApJ, 856, 79 [NASA ADS] [CrossRef] [Google Scholar]
  82. Yang, B., & Chen, H. 2019, ApJ, 874, 96 [Google Scholar]
  83. Yang, L., Yan, X., Xue, Z., et al. 2019a, ApJ, 887, 239 [Google Scholar]
  84. Yang, S., Zhang, J., Song, Q., et al. 2019b, ApJ, 878, 38 [NASA ADS] [CrossRef] [Google Scholar]
  85. Yashiro, S., Gopalswamy, N., Michalek, G., et al. 2004, J. Geophys. Res. (Space Phys.), 109, A07105 [NASA ADS] [CrossRef] [Google Scholar]
  86. Zarro, D. M., Sterling, A. C., Thompson, B. J., et al. 1999, ApJ, 520, L139 [Google Scholar]
  87. Zhang, J., Wang, J., Deng, Y., et al. 2001, ApJ, 548, L99 [NASA ADS] [CrossRef] [Google Scholar]
  88. Zhang, Q. M., Su, Y. N., & Ji, H. S. 2017, A&A, 598, A3 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  89. Zhou, G. P., Zhang, J., Wang, J. X., et al. 2017, ApJ, 851, L1 [Google Scholar]
  90. Zhou, G. P., Tan, C. M., Su, Y. N., et al. 2019, ApJ, 873, 23 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  91. Zou, P., Jiang, C., Wei, F., et al. 2020, ApJ, 890, 10 [CrossRef] [Google Scholar]
  92. Zuccarello, F., Romano, P., Farnik, F., et al. 2009, A&A, 493, 629 [Google Scholar]

Movies

Movie of Fig. 1 Access here

Movie of Fig. 2 Access here

Movie of Fig. 3 Access here

Movie of Fig. 6 Access here

All Figures

thumbnail Fig. 1.

Overview of the sympathetic eruptions of two filaments on 2015 November 15-16. (a1)–(a3): Sequence of GONG Hα images displaying evolutions of the two filaments (F1 and F2). The red and blue contours in panels (a1)–(a2) outline the filament fragments of F1 and F2, respectively. Ribbons produced by eruptive F1 and F2 and remanent F2 are denoted by arrows in panels (a2)–(a3). The GOES SXR 1–8 Å flux variation overlaid in panel (a3) reveals two B-class flares caused by eruptions of the two filaments. (b1)–(b3): Corresponding composite images of SDO/AIA 131 Å, 304 Å, and 171 Å channels. (c): Corresponding SDO/HMI LOS magnetogram. (d1)–(d2): Difference images from SOHO/LASCO C2 showing two successive CMEs driven by the sympathetic eruptions of F1 and F2. An animation of Hα, AIA composite, and LASCO C2 images, covering 21:30 UT on November 15 to 03:54 UT on November 16, is available online.
In the text
thumbnail Fig. 2.

Kinematic evolutions of eruptive F1 and the inward-spreading brightening on the south side of pre-eruption F2. (a1)–(a3): Sequence of AIA 304 Å images showing evolutions of F1 and two flare ribbons (NRF1 and SRF1). (a4): HMI LOS magnetogram superimposed with colored regions indicating positions of the evolving flare ribbons detected at different times in the 304 Å channel. (b1)–(b3): Enlarged 304 Å images displaying evolutions of SRF1 (dashed curves) and northward bright ribbon (IRF2) appearing on the south side of F2 (dotted curves). Green circles in (b3) indicate simultaneous brightenings on opposite sides of F2. (b4): Similar to (a4), but for the ribbons approaching F2 from two sides. (c1)–(c2): 171 Å and 131 Å images corresponding to (b3). (d): Variations in mean emission strength of the 304 Å passband within the regions N and S in (b1)–(b3). An associated animation of the 304 Å, 171 Å, and 131 Å images, covering 21:30 UT on November 15 to 00:30 UT on November 16, is available online.
In the text
thumbnail Fig. 3.

Coronal dimming on the south side of pre-eruption F2. (a1)–(a3): Sequence of AIA 193 Å images showing the appearance of coronal dimming on the south side of F2 before its eruption. The red and blue curves are contours of the HMI LOS magnetograms at ±50 G. The white curves outline the border of the dimming region around 00:10 UT on November 16. (b1)–(c3): Corresponding total EM and DEM-weighted average temperature maps exhibiting the evolution of plasma density and temperature in the dimming region. An associated animation of 193 Å images, covering 23:10 UT on November 15 to 00:10 UT on November 16, is available online.
In the text
thumbnail Fig. 4.

Three-dimensional (3D) magnetic fields above F1 and F2 revealed by NLFFF extrapolation at 22:00 UT on November 15. (a): Overlying loops of F1 and F2, forming a quadrupole magnetic field configuration. (b)–(c): Top view and side view of 3D distribution of magnetic field strength with values between 5 and 25 Gauss in the selected cube. (d)–(e): Distributions of magnetic field strength and decay index in the vertical plane based on the dark blue cut denoted in (a). The null point of the quadrupole magnetic configuration is distinctly depicted at a height of ∼90 Mm. (f): Height profiles of decay index averaged within two regions defined by two blue lines and two red lines in the vertical plane of (e), respectively.
In the text
thumbnail Fig. 5.

NLFFF extrapolation results derived from the photospheric vector field of 00:00 UT on November 16.
In the text
thumbnail Fig. 6.

Partial eruption of F2. (a)–(c): 304 Å and Hα images showing partial eruption of F2. Green arrows in (a) denote eruptive direction of the west part of F2. Green ellipse in (b) marks a bending structure in the middle part of F2 during its rapid rising phase. White curves in (a)–(b) delineate the axis of eruptive F2. (d)–(f): 131 Å, 171 Å images, and difference image of 304 Å corresponding to (b). Green arrows in (d) and (e) represent southeastward motion of the activated material of the east part of F2. The colored arrows in (f) represent the horizontal velocity fields of filament material with values larger than 30 km s−1 derived from 304 Å images through LCT method. (g)–(h): Time-distance plots derived from the 304 Å images along lines “A–B” and “C–D” shown in (a). The dotted oblique line in (g) delineates linear fitting of the front of eruptive F2 in its rapid rising phase. An associated animation of 304 Å, 171 Å, and 131 Å images, covering 23:50 UT on November 15 to 03:59 UT on November 16, is available online.
In the text

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